Risk Cross Sections and Their Application to Risk Estimation in the Galactic Cosmic-Ray Environment

1995 ◽  
Vol 141 (1) ◽  
pp. 57 ◽  
Author(s):  
Stanley B. Curtis ◽  
John E. Nealy ◽  
John W. Wilson
Keyword(s):  
Cross Sections ◽  
Risk Estimation ◽  
Cosmic Ray ◽  
Galactic Cosmic Ray

scholarly journals Impact of cross sections uncertainties on the study of galactic cosmic-ray propagation with the DRAGON2 code

2021 ◽  
Author(s):  
Pedro De la Torre Luque ◽  
M. Nicola Mazziotta ◽  
Fabio Gargano ◽  
Francesco Loparco ◽  
Davide Serini
Keyword(s):  
Cross Sections ◽  
Cosmic Ray ◽  
Galactic Cosmic Ray

scholarly journals Combined analysis of AMS-02 (Li,Be,B)/C, N/O, 3He, and 4He data

2020 ◽  
Vol 639 ◽  
pp. A131 ◽  
Author(s):  
N. Weinrich ◽  
Y. Génolini ◽  
M. Boudaud ◽  
L. Derome ◽  
D. Maurin
Keyword(s):  
Cross Sections ◽  
Production Cross ◽  
Cosmic Ray ◽  
Nuclear Data ◽  
Quantitative Agreement ◽  
Propagation Model ◽  
Solar Modulation ◽  
Combined Analysis ◽  
Correlation Lengths ◽  
Galactic Cosmic Ray

Context. The Alpha Magnetic Spectrometer (AMS-02) measured several secondary-to-primary ratios enabling a detailed study of Galactic cosmic-ray transport. Aims. We constrain previously derived benchmark scenarios (based on AMS-02 B/C data only) using other secondary-to-primary ratios to test the universality of transport and the presence of a low-rigidity diffusion break. Methods. We use the 1D thin disc/thick halo propagation model of USINE V3.5 and a χ2 minimisation accounting for a covariance matrix of errors (AMS-02 systematics) and nuisance parameters (cross-sections and solar modulation uncertainties). Results. The combined analysis of AMS-02 Li/C, Be/C, and B/C strengthens the case for a diffusion slope of δ = 0.50 ± 0.03 with a low-rigidity break or upturn of the diffusion coefficient at GV rigidities. Our simple model can successfully reproduce all considered data (Li/C, Be/C, B/C, N/O, and 3He/4He), although several issues remain: (i) the quantitative agreement depends on the assumptions made on the poorly constrained correlation lengths of AMS-02 data systematics; (ii) combined analyses are very sensitive to production cross-sections, and we find post-fit values differing by ∼5 − 15% from their most likely values (roughly within currently estimated nuclear uncertainties); (iii) two very distinct regions of the parameter space remain viable, either with reacceleration and convection, or with purely diffusive transport. Conclusions. To take full benefit of combined analyses of AMS-02 data, better nuclear data and a better handle on energy correlations in the data systematic are required. AMS-02 data on heavier species are eagerly awaited to explore cosmic-ray propagation scenarios further.

scholarly journals Modeling of the Near-Earth Low-Energy Antiproton Fluxes

2011 ◽  
Vol 2011 ◽  
pp. 1-6
Author(s):  
U. B. Jayanthi ◽  
A. A. Gusev
Keyword(s):  
Cross Sections ◽  
Particle Production ◽  
Solar Maximum ◽  
Cosmic Ray ◽  
Field Approximation ◽  
Solar Modulation ◽  
Inner Magnetosphere ◽  
Model Code ◽  
Antiproton Production ◽  
Galactic Cosmic Ray

The local interstellar antiproton spectrum is simulated taking into account antineutron decay, (He,p) interaction, secondary and tertiary antiproton production, and the solar modulation in the “force field” approximation. Inclusive invariant cross-sections were obtained through a Monte Carlo procedure using the Multistage Dynamical Model code simulating various processes of the particle production. The results of the simulations provided flux values of to and to antiprotons/( s sr GeV) at energies of 0.2 and 1 GeV, respectively, for the solar maximum and minimum epochs. Simulated flux of the trapped antiprotons in the inner magnetosphere due to galactic cosmic ray (GCR) interactions with the atmospheric constituents exceeds the galactic antiproton flux up to several orders. These simulation results considering the assumptions with the attendant limitations are in comprehensive agreement with the experimental data including the PAMELA ones.

scholarly journals The theory of cosmic ray scattering on pre-existing MHD modes meets data

2021 ◽  
Vol 502 (4) ◽  
pp. 5821-5838
Author(s):  
Ottavio Fornieri ◽  
Daniele Gaggero ◽  
Silvio Sergio Cerri ◽  
Pedro De La Torre Luque ◽  
Stefano Gabici
Keyword(s):  
Diffusion Coefficients ◽  
Galactic Halo ◽  
Dominant Role ◽  
Cosmic Ray ◽  
High Energy ◽  
Scattering Rate ◽  
Equilibrium Spectrum ◽  
Galactic Cosmic Ray ◽  
Comprehensive Study ◽  
Ray Scattering

ABSTRACT We present a comprehensive study about the phenomenological implications of the theory describing Galactic cosmic ray scattering on to magnetosonic and Alfvénic fluctuations in the GeV−PeV domain. We compute a set of diffusion coefficients from first principles, for different values of the Alfvénic Mach number and other relevant parameters associated with both the Galactic halo and the extended disc, taking into account the different damping mechanisms of turbulent fluctuations acting in these environments. We confirm that the scattering rate associated with Alfvénic turbulence is highly suppressed if the anisotropy of the cascade is taken into account. On the other hand, we highlight that magnetosonic modes play a dominant role in Galactic confinement of cosmic rays up to PeV energies. We implement the diffusion coefficients in the numerical framework of the dragon code, and simulate the equilibrium spectrum of different primary and secondary cosmic ray species. We show that, for reasonable choices of the parameters under consideration, all primary and secondary fluxes at high energy (above a rigidity of $\simeq 200 \, \mathrm{GV}$) are correctly reproduced within our framework, in both normalization and slope.

A comparison of catalogues of Forbush decreases identified from individual and a network of neutron monitors: a critical perspective

2021 ◽  
Vol 503 (4) ◽  
pp. 5675-5691
Author(s):  
O Okike ◽  
J A Alhassan ◽  
E U Iyida ◽  
A E Chukwude
Keyword(s):  
Cosmic Ray ◽  
Radiowave Propagation ◽  
Current Work ◽  
Survey Method ◽  
Critical Perspective ◽  
Short Term ◽  
Forbush Decreases ◽  
Academy Of Sciences ◽  
Galactic Cosmic Ray ◽  
Monitor Data

ABSTRACT Short-term rapid depressions in Galactic cosmic ray (GCR) flux, historically referred to as Forbush decreases (FDs), have long been recognized as important events in the observation of cosmic ray (CR) activity. Although theories and empirical results on the causes, characteristics, and varieties of FDs have been well established, detection of FDs, from either isolated detectors' or arrays of neutron monitor data, remains a subject of interest. Efforts to create large catalogues of FDs began in the 1990s and have continued to the present. In an attempt to test some of the proposed CR theories, several analyses have been conducted based on the available lists. Nevertheless, the results obtained depend on the FD catalogues used. This suggests a need for an examination of consistency between FD catalogues. This is the aim of the present study. Some existing lists of FDs, as well as FD catalogues developed in the current work, were compared, with an emphasis on the FD catalogues selected by the global survey method (GSM). The Forbush effects and interplanetary disturbances database (FEID), created by the Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radiowave Propagation Russian Academy of Sciences (IZMIRAN), is the only available comprehensive and up to date FD catalogue. While there are significant disparities between the IZMIRAN FD and other event lists, there is a beautiful agreement between FDs identified in the current work and those in the FEID. This may be a pointer to the efficiency of the GSM and the automated approach to FD event detection presented here.

scholarly journals Galactic cosmic ray origin sites: Supernova remnants and superbubbles

2012 ◽  
Author(s):  
A. M. Bykov ◽  
D. C. Ellison ◽  
P. E. Gladilin ◽  
S. M. Osipov
Keyword(s):  
Supernova Remnants ◽  
Cosmic Ray ◽  
Galactic Cosmic Ray
Sign in / Sign up

Export Citation Format

Share Document